718 research outputs found
Classical Analogue of the Ionic Hubbard Model
In our earlier work [M. Hafez, {\em et al.}, Phys. Lett. A {\bf 373} (2009)
4479] we employed the flow equation method to obtain a classic effective model
from a quantum mechanical parent Hamiltonian called, the ionic Hubbard model
(IHM). The classical ionic Hubbard model (CIHM) obtained in this way contains
solely Fermionic occupation numbers of two species corresponding to particles
with \up and \down spin, respectively. In this paper, we employ the
transfer matrix method to analytically solve the CIHM at finite temperature in
one dimension. In the limit of zero temperature, we find two insulating phases
at large and small Coulomb interaction strength, , mediated with a gap-less
metallic phase, resulting in two continuous metal-insulator transitions. Our
results are further supported with Monte Carlo simulations.Comment: 12 figure
Nonlinear Jaynes-Cummings model of atom-field interaction
Interaction of a two-level atom with a single mode of electromagnetic field
including Kerr nonlinearity for the field and intensity-dependent atom-field
coupling is discussed. The Hamiltonian for the atom-field system is written in
terms of the elements of a closed algebra, which has
SU(1,1) and Heisenberg-Weyl algebras as limiting cases. Eigenstates and
eigenvalues of the Hamiltonian are constructed.
With the field being in a coherent state initially, the dynamical behaviour
of atomic-inversion, field-statistics and uncertainties in the field
quadratures are studied. The appearance of nonclassical features during the
evolution of the field is shown. Further, we explore the overlap of initial and
time-evolved field states.Comment: 14 pages, 6 figures is PS forma
Antifungal susceptibility, genotyping, resistance mechanism, and clinical profile of <i>Candida tropicalis</i> blood isolates
Antifungal susceptibility, genotyping, resistance mechanism, and clinical profile of <i>Candida tropicalis</i> blood isolates
Indikatoren einer tiergerechten Mastputenhaltung unter den Bedingungen der ökologischen Geflügelmast
Ziel der Studie war eine Analyse der Häufigkeit und des Ausprägungsgrades tierschutzrelevanter Veränderungen bei Puten, die gemäß den Bedingungen der EU-Verordnung 889/2008 für den ökologischen Landbau gehalten wurden. In zwei Durchgängen wurden in neun Aufzucht- und 14 Mastbetrieben 32 Herden mit insgesamt 105.483 Tieren erfasst. Der Tiergesundheitsstatus der einzelnen Herden wurde stichprobenartig an fünf Zeitpunkten durch Beurteilung von 60 Einzeltieren dokumentiert. Bei jedem Bestandsbesuch wurden außerdem Einstreuproben entnommen und ihr Feuchtigkeitsgehalt thermogravimetrisch bestimmt.
Die mittlere kumulierte Verlustrate in der Aufzuchtphase lag bei 3,3 % und in der 16. Lebenswoche bei 4,5%. Am Ende der Aufzuchtphase wiesen bis zu 44 % der untersuchten Tiere Epithelnekrosen an den Fußballen auf. Häufigkeit und Schweregrad von Ballenveränderungen nahmen im Verlauf der Mastphase weiter zu. So wurden in der 16. Lebenswoche bei über 80 % der untersuchten Puten Ballennekrosen festgestellt.
Am Schlachthof erfolgte eine Aufnahme allgemeiner Daten zur Schlachtung und folgend die visuelle Beschau von 60 Puten je Herde. Der überwiegende Teil der Tiere (97,7%) wies zum Zeitpunkt der Schlachtung Veränderungen der Fußballen auf, während Brusthautveränderungen nur selten dokumentiert wurden. Vermehrt traten weiterhin Leberveränderungen, insbesondere Grünfärbungen auf, wobei deutliche Unterschiede zwischen verschiedenen Betrieben sowie zwischen den einzelnen Durchgängen festgestellt wurden. Auch Gelenksveränderungen waren häufige Befunde.
Als ein maßgeblicher Faktor für die Gesunderhaltung eines Putenbestandes ist die Befähigung des bestandsbetreuenden Personenkreises anzusehen, gesundheitliche Probleme frühzeitig zu erkennen und zeitnah darauf zu reagieren. Neben der Qualität des Einstreusubstrates inklusive Beurteilung der Kotkonsistenz können Häufigkeit und Ausprägung von Ballenveränderungen wertvolle Hinweise für eine Einschätzung des Tierhaltungsstandards in einem Bestand liefern und sind als wichtige, einfach erfassbare Tierschutzindikatoren einzustufen . Auch Gelenks- und Leberveränderungen sind aufgrund hoher Prävalenzen als relevante Tiergesundheitsparameter zu betrachten, die im Rahmen eines Monitorings routinemäßig erfasst werden sollten
CMB observations from the CBI and VSA: A comparison of coincident maps and parameter estimation methods
We present coincident observations of the Cosmic Microwave Background (CMB)
from the Very Small Array (VSA) and Cosmic Background Imager (CBI) telescopes.
The consistency of the full datasets is tested in the map plane and the Fourier
plane, prior to the usual compression of CMB data into flat bandpowers. Of the
three mosaics observed by each group, two are found to be in excellent
agreement. In the third mosaic, there is a 2 sigma discrepancy between the
correlation of the data and the level expected from Monte Carlo simulations.
This is shown to be consistent with increased phase calibration errors on VSA
data during summer observations. We also consider the parameter estimation
method of each group. The key difference is the use of the variance window
function in place of the bandpower window function, an approximation used by
the VSA group. A re-evaluation of the VSA parameter estimates, using bandpower
windows, shows that the two methods yield consistent results.Comment: 10 pages, 6 figures. Final version. Accepted for publication in MNRA
Radio source calibration for the VSA and other CMB instruments at around 30 GHz
Accurate calibration of data is essential for the current generation of CMB
experiments. Using data from the Very Small Array (VSA), we describe procedures
which will lead to an accuracy of 1 percent or better for experiments such as
the VSA and CBI. Particular attention is paid to the stability of the receiver
systems, the quality of the site and frequent observations of reference
sources. At 30 GHz the careful correction for atmospheric emission and
absorption is shown to be essential for achieving 1 percent precision. The
sources for which a 1 percent relative flux density calibration was achieved
included Cas A, Cyg A, Tau A and NGC7027 and the planets Venus, Jupiter and
Saturn. A flux density, or brightness temperature in the case of the planets,
was derived at 33 GHz relative to Jupiter which was adopted as the fundamental
calibrator. A spectral index at ~30 GHz is given for each. Cas A,Tau A, NGC7027
and Venus were examined for variability. Cas A was found to be decreasing at
percent per year over the period March 2001 to August 2004.
In the same period Tau A was decreasing at percent per year. A
survey of the published data showed that the planetary nebula NGC7027 decreased
at percent per year over the period 1967 to 2003. Venus showed
an insignificant ( percent) variation with Venusian illumination.
The integrated polarization of Tau A at 33 GHz was found to be
percent at pa .}Comment: 13 pages, 15 figures, submitted to MNRA
Cosmological parameter estimation using Very Small Array data out to l=1500
We estimate cosmological parameters using data obtained by the Very Small
Array (VSA) in its extended configuration, in conjunction with a variety of
other CMB data and external priors. Within the flat CDM model, we find
that the inclusion of high resolution data from the VSA modifies the limits on
the cosmological parameters as compared to those suggested by WMAP alone, while
still remaining compatible with their estimates. We find that , , , , and
for WMAP and VSA when no external prior is
included.On extending the model to include a running spectral index of density
fluctuations, we find that the inclusion of VSA data leads to a negative
running at a level of more than 95% confidence (),
something which is not significantly changed by the inclusion of a stringent
prior on the Hubble constant. Inclusion of prior information from the 2dF
galaxy redshift survey reduces the significance of the result by constraining
the value of . We discuss the veracity of this result in the
context of various systematic effects and also a broken spectral index model.
We also constrain the fraction of neutrinos and find that at
95% confidence which corresponds to when all neutrino
masses are the equal. Finally, we consider the global best fit within a general
cosmological model with 12 parameters and find consistency with other analyses
available in the literature. The evidence for is only marginal
within this model
The influence of the fasting period on the number of nymphal instars and on the sex ratio of Argas (Persicargas) miniatus (Acari: Argasidae)
High sensitivity measurements of the CMB power spectrum with the extended Very Small Array
We present deep Ka-band ( GHz) observations of the CMB made
with the extended Very Small Array (VSA). This configuration produces a
naturally weighted synthesized FWHM beamwidth of arcmin which covers
an -range of 300 to 1500. On these scales, foreground extragalactic
sources can be a major source of contamination to the CMB anisotropy. This
problem has been alleviated by identifying sources at 15 GHz with the Ryle
Telescope and then monitoring these sources at 33 GHz using a single baseline
interferometer co-located with the VSA. Sources with flux densities \gtsim 20
mJy at 33 GHz are subtracted from the data. In addition, we calculate a
statistical correction for the small residual contribution from weaker sources
that are below the detection limit of the survey.
The CMB power spectrum corrected for Galactic foregrounds and extragalactic
point sources is presented. A total -range of 150-1500 is achieved by
combining the complete extended array data with earlier VSA data in a compact
configuration. Our resolution of allows the first 3
acoustic peaks to be clearly delineated. The is achieved by using mosaiced
observations in 7 regions covering a total area of 82 sq. degrees. There is
good agreement with WMAP data up to where WMAP data run out of
resolution. For higher -values out to , the agreement in
power spectrum amplitudes with other experiments is also very good despite
differences in frequency and observing technique.Comment: 16 pages. Accepted in MNRAS (minor revisions
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